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| __NOTOC__
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| {{Planetbox begin
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| | name = [[Harvard Revised catalogue|HR]] 8799 c
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| }}
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| {{Planetbox image
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| | image = Exoplanet Comparison HR 8799 c.png
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| | caption = Size comparison of HR 8799 c (gray) with Jupiter.
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| }}
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| {{Planetbox star
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| | star = [[HR 8799]]
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| | constell = [[Pegasus (constellation)|Pegasus]]
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| | RA = {{RA|23|07|28.7150}}<ref name="SIMBAD">{{SIMBAD link|HR+8799|V* V342 Peg -- Variable Star of gamma Dor type}}, entry, [[SIMBAD]]. Accessed on line November 14, 2008.</ref>
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| | DEC = {{DEC|+21|08|03.302}}<ref name="SIMBAD" />
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| | app_mag = 5.964<ref name="SIMBAD" />
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| | dist_ly = 129 ± 4<ref name="vanLeeuwen2007">{{cite web|url=http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=113804|title=HIP 114189|work=Hipparcos, the New Reduction|author=van Leeuwen, F.|year=2007|accessdate=2008-10-13}}</ref><ref group="note" name="calculate_distance">Computed from parallax: <math>\scriptstyle \mathrm{distance\ in\ parsecs}=\frac{1000}{\mathrm{parallax\ in\ milliarcseconds}}</math></ref>
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| | dist_pc = 39 ± 1<ref name="vanLeeuwen2007" /><ref group="note" name="calculate_distance" />
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| | class = kA5 hF0 mA5 V; λ Boo<ref name="Gray1999">{{cite journal|title=HR 8799: A Link between γ Doradus Variables and λ Bootis Stars|author=Gray, R.O. and Kaye, A.B.|year=1999|journal=[[The Astronomical Journal]]|volume=118|issue=6|pages=2993–2996|doi=10.1086/301134|bibcode=1999AJ....118.2993G}}</ref><ref name="Kaye1999">{{cite journal|title=Gamma Doradus Stars: Defining a New Class of Pulsating Variables|author=Kaye, A.B. ''et al.''|year=1999|journal=[[PASP]]|volume=111|issue=761|pages=840–844|bibcode=1999PASP..111..840K|doi=10.1086/316399|arxiv = astro-ph/9905042 }}</ref>
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| }}
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| {{Planetbox separation
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| | epoch = 2008-09-18
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| | separation_mas = 964<ref name="Marois2008">{{cite journal |last=Marois |first=Christian |authorlink= |coauthors=''et al.'' |date=November 2008 |title=Direct Imaging of Multiple Planets Orbiting the Star HR 8799 |journal=[[Science (journal)|Science]] |volume=322 |issue=5906 |pages=1348–1352 |doi=10.1126/science.1166585 |arxiv=0811.2606 |accessdate= |quote= |pmid=19008415 |bibcode = 2008Sci...322.1348M }}</ref><ref group="note" name="separation">Calculated from the separations in the East and North directions which are −0.657 and 0.706 [[arcsecond]]s respectively.</ref>
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| | position_angle = 317.06<ref name="Marois2008" /><ref group="note" name="separation" />
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| | separation = 38<ref name="Marois2008" />
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| }}
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| {{Planetbox orbit
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| | semimajor = ~ 38<ref name="Marois2008" /><ref group="note" name="circular_orbit">Value given assuming the planet's orbit is circular and is being observed face-on.</ref>
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| | semimajor_gm = ~ 5600
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| | period_year = ~ 190<ref name="Marois2008" /><ref group="note" name="circular_orbit" />
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| }}
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| {{Planetbox character
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| | mass = 7{{±|3|2}}<ref>{{cite arxiv |eprint=1011.4918 |author1=Marois |author2=Zuckerman |author3=Konopacky |author4=Macintosh |author5=Barman |title=Images of a fourth planet orbiting HR 8799 |class=astro-ph.EP |year=2010}}</ref>
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| | radius = 1.3<ref name="spectrum"/>
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| | density = 3.2{{±|1.3|0.7}}
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| | temperature = 1090{{±|10|90}}<ref name="Marois2008" />
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| }}
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| {{Planetbox discovery
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| | discovery_date = November 13, 2008
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| | discoverers = Marois ''et al.''
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| | discovery_method = [[Direct imaging]]
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| | discovery_site = [[W.M. Keck Observatory|Keck]] and [[Gemini Observatory|Gemini<br/>observatories]] in [[Hawaii]]
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| | discovery_status = Published
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| }}
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| {{Planetbox catalog
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| | names = [[Henry Draper catalogue|HD]] 218396 c<ref>{{SIMBAD link|HD+218396c|HD 218396c -- Extra-solar Planet Candidate}}, entry, [[SIMBAD]]. Accessed on line December 6, 2008.</ref>
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| }}
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| {{Planetbox reference
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| | star = HR+8799
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| | planet = c
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| | simbad = HD+218396c
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| }}
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| {{Planetbox end}}
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| '''HR 8799 c''' is an [[extrasolar planet]] located approximately 129 [[light-year]]s away in the [[constellation]] of [[Pegasus (constellation)|Pegasus]], orbiting the 6th [[apparent magnitude|magnitude]] [[Lambda Boötis star]] [[HR 8799]]. This planet has a mass between 5 and 10 [[Jupiter mass]]es and a radius from 20 to 30% larger than [[Jupiter]]'s. It orbits at 38 [[astronomical units|AU]] from HR 8799 with an unknown eccentricity and a period of 190 years; it is the 2nd planet discovered in the HR 8799 system. Along with two other planets orbiting HR 8799, this planet was discovered on November 13, 2008 by Marois ''et al.'', using the [[W.M. Keck Observatory|Keck]] and the [[Gemini Observatory|Gemini observatories]] in [[Hawaii]]. These planets were discovered using the [[direct imaging]] technique.<ref name="Marois2008" /><ref>{{cite press release|url=http://www.keckobservatory.org/article.php?id=231|title=Astronomers capture first images of newly-discovered solar system|publisher=W. M. Keck Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite press release|url=http://www.gemini.edu/node/11151|title=Gemini Releases Historic Discovery Image of Planetary First Family|publisher=Gemini Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite news|title=Scientists Publish First Direct Images of Extrasolar Planets|first=Joel|last=Achenbach|work=[[The Washington Post]]|publisher=[[The Washington Post Company]]|date=2008-11-13|accessdate=2008-12-02|url=http://www.washingtonpost.com/wp-dyn/content/article/2008/11/13/AR2008111302267.html}}</ref><ref>{{cite journal |title=Stability of the directly imaged multiplanet system HR 8799: resonance and masses |author=Fabrycky ''et al.'' |date=1 December 2008|pages=1408–1421 |accessdate=2008-12-02 |issue=2 |volume=710 |author2=Murray-Clay |doi=10.1088/0004-637X/710/2/1408 |journal=Astrophys.J. |arxiv=0812.0011|bibcode = 2010ApJ...710.1408F }}</ref> In January 2010, HR 8799 c became the 3rd exoplanet to have a portion of its spectrum directly observed (following 2M1207b and 1RXS J1609b), confirming the feasibility of direct spectrographic studies of exoplanets.<ref name="spectrum"/><ref>{{cite journal|last=Janson|first=M.|date=13 January 2010|title=VLT Captures First Direct Spectrum of an Exoplanet|journal=ESO|location=La Silla Observatory|url=http://www.eso.org/public/news/eso1002/|accessdate=2010-01-13}}</ref>
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| ==Spectra==
| | Bonus: WP Twin and WP Twin Auto Backup: (link to ) While not a theme, I think this software is essential if you are maintaining your Wordpress blog or regularly create new blog sites. Thus, it is important to keep pace with this highly advanced age and have a regular interaction with your audience to keep a strong hold in the business market. If you have any concerns regarding the place and how to use [http://miu.tw/wordpress_backup_plugin_540126 wordpress backup plugin], you can call us at our own web-site. The effect is to promote older posts by moving them back onto the front page and into the rss feed. Donor oocytes and menopausal pregnancy: Oocyte donation to women of advanced reproductive age: pregnancy results and obstetrical outcomes in patients 45 years and older. If you are happy with your new look then click "Activate 'New Theme'" in the top right corner. <br><br>Most Word - Press web developers can provide quality CMS website solutions and they price their services at reasonable rates. Best of all, you can still have all the functionality that you desire when you use the Word - Press platform. This plugin allows a blogger get more Facebook fans on the related fan page. From my very own experiences, I will let you know why you should choose WPZOOM Live journal templates. Moreover, many Word - Press themes need to be purchased and designing your own WP site can be boring. <br><br>Minor and medium sized corporations also have a lot to obtain by shelling out in a very good website. Browse through the popular Wordpress theme clubs like the Elegant Themes, Studio Press, Woo - Themes, Rocket Theme, Simple Themes and many more. Use this section to change many formatting elements. In crux the developer must have a detailed knowledge not only about the marketing tool but also about the ways in which it can be applied profitably. After that the developer adds the unordered list for navigations. <br><br>The next thing I did after installing Wordpress was to find myself a free good-looking Wordpress-theme offering the functionality I was after. php file in the Word - Press root folder and look for this line (line 73 in our example):. Websites that do rank highly, do so becaue they use keyword-heavy post titles. If you just want to share some picture and want to use it as a dairy, that you want to share with your friends and family members, then blogger would be an excellent choice. If your site does well you can get paid professional designer to create a unique Word - Press theme. <br><br>Instead, you can easily just include it with our bodies integration field in e - Panel. If you operate a website that's been built on HTML then you might have to witness traffic losses because such a site isn't competent enough in grabbing the attention of potential consumers. Useful Plugins Uber - Menu Top Megamenu Now it is the time of sticky Top navbar. Change the entire appearance of you blog using themes with one click. As for performing online business, websites and blogs are the only medium that are available to interact with customers and Word - Press perform this work with the help of cross-blog communication tools, comments and full user registration plug-ins. |
| [[File:Spectrum of planet around HR 8799 (annotated).jpg|thumb|left|alt=Spectrum of planet around HR8799. Credit: ESO/M. Janson.|The spectrum of the planet HR 8799 c. The spectrum of the star and the planet was obtained with the NACO adaptive optics instrument on [[European Southern Observatory|ESO]]’s [[Very Large Telescope]].]]
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| Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Obervatory show evidence of Ammonia, perhaps some Acetylene but neither Carbon Dioxide nor substantial Methane.<ref name=Gilliland>{{cite web|first = B. R. Oppenheimer|title= Reconnaissance of the HR 8799 Exosolar System I: Near IR Spectroscopy|url=http://arxiv.org/abs/1303.2627|publisher=Cornell University|accessdate=12 March 2013}}</ref>
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| High resolution spectroscopy with the OSIRIS instrument on the Keck Observatory show numerous well resolved lines of molecular absorption in the planet's atmosphere in the K band. Although methane is absent, the planet's atmosphere contains both water and carbon monoxide; the carbon-to-oxygen ratio of HR 8799 c is higher than that of its star, suggesting that the planet formed through the core accretion process.<ref>[http://www.salon.com/2013/03/14/alien_planets_atmosphere_contains_water_and_carbon_monoxide/ Alien planet’s atmosphere contains water and carbon monoxide ]</ref><ref>[http://www.space.com/20230-giant-planet-atmosphere-solar-system.html Giant Alien Planet in Supersized Solar System May Solve Mystery]</ref>
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| ==Notes==
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| <references group="note" /> | |
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| ==See also==
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| * [[Fomalhaut b]]
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| | |
| ==References==
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| {{reflist|refs=
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| <ref name="spectrum">
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| {{cite journal |last=Jason |first=M. |coauthors=C. Bergfors, M. Goto, W. Brandner, D. Lafrenière |year=2010 |title=Spatially resolved spectroscopy of the exoplanet HR 8799 c |journal=The Astrophysical Journal |volume= |issue= |pages= |url=http://www.eso.org/public/archives/releases/sciencepapers/eso1002/eso1002.pdf |doi= |accessdate=2010-01-13}}</ref>
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| }}
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| ==External links==
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| {{Commons category-inline}}
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| * {{cite web | url=http://media4.obspm.fr/exoplanets/base/planete.php?etoile=HR+8799&planete=c | title=HR 8799 c | work=Exoplanets}}
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| | |
| {{HR 8799}}
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| {{Sky|23|07|28.7150|+|21|08|03.302|129}}
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| {{DEFAULTSORT:Hr 8799 C}}
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| [[Category:HR 8799]]
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| [[Category:Exoplanets discovered in 2008]]
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| [[Category:Gas giants]]
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| [[Category:Pegasus (constellation)]]
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| [[Category:Exoplanets detected by direct imaging]]
| |
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